Nucleosynthesis in Type I X-ray bursts (XRB) proceeds eventually through the rp-process near the proton drip-line. Astrophysical calculations of XRB light curves depend upon the theoretical modelling of the beta decays of interest, with the N=Z: 64Ge, 68Se, 72Kr, 76Sr being key nuclei in this context. Several such theoretical calculations have shown that, in these high-density and high-temperature scenarios, continuum electron capture and decay rates from excited states play an important role, in particular for nuclear species at and around the waiting-point nuclei. In this presentation I will introduce the basics of the XRBs and the rp-process, and will show how we measure the beta decay of the key N=Z waiting point nuclei and their N=Z+2 second-neighbours, with the main goal of determining the B(GT) distribution for these decays. These measurements provide a benchmark for testing and constraining models under terrestrial conditions that are used later for predictions in stellar environments.
IFIC Experimental Seminar organizers